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Date and Time of the Query: 2018-12-09 T18:14:35 PST
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Notes for object NGC 4414

16 note(s) found in NED.


1. 2008ApJ...677..926S
Re:NGC 4414
NGC 4414 is a relatively isolated, flocculent Sc galaxy (de Vaucouleurs et al.
1976) that is optically classified as a transition object with no broad lines
detected (H97). Therefore, there is no firm evidence for an AGN based solely on
its optical spectrum. Its optical line ratios are very close to the Kewley et
al. (2001) starburst theoretical-limit line, as can be seen in Figure 1. There
are no published observations of NGC 4414 suggesting that it contains an AGN.
This source was not detected at radio frequencies by Filho et al. (2006), and
arcsecond-resolution VLA observations reveal a diffuse radio morphology (Filho
et al. 2000). There is also no indication of intense nuclear star formation.
Based on its infrared and H{alpha} luminosities, it is not classified as a
starburst. In fact, H{alpha} images show a central hole, indicating that there
is no nuclear star formation (Pogge 1989) in this galaxy. Although there is no
evidence for powerful star formation activity, H I and CO observations indicate
that it has one of the highest disk neutral surface gas densities known (Braine
et al. 1993). The central stellar velocity dispersion in this galaxy is 128 +/-
9 km s^-1^ (Barth et al. 2002).

2. 2007ApJS..173..538T
Re:NGC 4414
NGC 4414 (Fig. 16.21).-A member of the Coma I group (dominated by NGC 4631), our
observations of this SA(rs)c? LINER galaxy reveal a bright main disk surrounded
by XUV clumps distributed in disorganized (tightly wrapped?) spiral features at
almost all position angles. The clumps are not located at extreme galactocentric
distances, but rather tend to hug the main disk. This galaxy is one of the few
to have confirmed outer disk molecular clouds (Braine & Herpin 2004) at a
limited number of positions near H I peaks (Thornley & Mundy 1997). Deep
H{alpha} imaging reveals sporadic H II regions coinciding with some of the XUV
clumps (Gavazzi et al. 2003, 2006). SDSS imagery allows one to see the brightest
XUV-disk stellar complexes. Despite belonging to the Coma I group, NGC 4414 is
dynamically isolated in the sense that it has no known tidally perturbing
companion.

3. 2005MNRAS.357..361S
Re:NGC 4414
NGC 4414. This mid-inclination spiral (i= 54^deg^) is thought to be in front of
the Virgo cluster. It has two central peaks which are best explained as the
enhanced line-of-sight column densities seen through a ring orbiting the
galactic core. The ~30-arcsec separation of the peaks corresponds to a linear
distance of 2.1 kpc at the assumed distance to NGC 4414. The idea of a dusty
ring surrounding the core is supplemented by the molecular gas hole detected in
the same region by Sakamoto et al. (1999).

4. 2002ApJS..143...73E
Re:NGC 4414
NGC 4414.---Sab: Bright nuclear point source embedded in a small
elliptical bulge. Inner disk has a different P.A. than the bulge.
Spiral features appear in the inner disk and are brightest here. The
disk is very knotty, with evidence for many bits of arms. Spiral
pattern is flocculent.

5. 2001A&A...368...16M
Re:NGC 4414
32. NGC 4414 is a multi-armed flocculent Sc spiral of medium inclination
in the Virgo cluster. We obtained good fit residua. In the HST key project
the Cepheid distance of NGC 4414 was determined to 19.1 Mpc (Turner et al.
1998).

6. 2000ApJS..129...93F
Re:NGC 4414
NGC 4414. - We detect ~ 29 mJy of low surface brightness emission,
distributed along ~ 1.5', in a structure aligned with the galaxy's major
axis. NVSS detected a 242 mJy source, while FIRST detected a
double-peaked source with 44 and 64 mJy components. The Condon (1983)
1.465 GHz, 12.5" resolution map and the Condon (1987) 1.49 GHz, 1.0'
resolution map show comparable north-south structure, measuring
~ 0.22 Jy. Using this last value plus the 78 mJy measured at 4.85 GHz,
15" resolution, Condon et al. (1991) obtain a steep spectral index.

7. 1999ApJS..124..403S
Re:NGC 4414
5.9. NGC 4414
NGC 4414 has flocculent spiral arms and active star-forming regions
spread over the disk. The gas distribution is close to axisymmetric and
the velocity field is almost circular, probably owing to the weakness of
the density waves. The large gas hole of ~ 1 kpc diameter at the center
is exceptional in our sample. Unlike gas holes in the centers of other
galaxies (e.g., IC 342 and NGC 1530), the central gas hole in NGC 4414
is apparently not related to a bar. Giant molecular cloud associations
(GMAs) in the gas disk have been discussed in detail by Sakamoto (1996a)
and Thornley & Mundy (1997b). The CO channel maps used to make the
moment maps are in Sakamoto (1996a).

8. 1996ApJ...469L..45T
Re:NGC 4414
NGC 4414.--The high gas surface density Scd galaxy NGC 4414 (Braine, Combes, &
van Driel 1993) is 2.5 times more distant than NGC 3521 (Pierce 1994) and
remains the most flocculent of the sample in K' emission. Comparison with
H{alpha} imaging suggests that much of the residual K' emission in the inner
disk (Fig. 3c) can be traced to the distribution of H II regions in NGC 4414;
for example, bright star-forming regions to the northwest and southeast of the
nucleus likely contribute to an apparent NIR ring/arm structure of radius 20"
(2 kpc). Outer "arm" segments to the north and south extend to a radius of
~40" (0.4 R_25_) and are continuous over 60^deg^ in azimuth. While these
outer structures are similar in linear scale to the arm structures seen in
NGC 3521 and NGC 5055, they do not appear to contribute to a regular two-arm
spiral pattern.

9. 1994CAG1..B...0000S
Re:NGC 4414
Sc(sr)II.2
H-2384-H
Feb 21/22, 1947
IIaO
10 min
The multiple-armed spiral structure is well
developed in NGC 4414. Dust accompanies the
luminous arm fragments and is well silhouetted
against the near side of the underlying disk. The
HII regions are unresolved, as are the brightest
stars on this plate taken with the Mount Wilson
100-inch Hooker reflector. The redshift of NGC 4414
is v_o = 702 km/s.

10. 1993A&AS...97..887B
Re:NGC 4414
NGC 4414
Because of the low spatial resolution of the 14m FCRAO and 12m NRAO
telescopes at 115 GHz, S88 and Sage & Isbell (1991) did not detect the
powerful molecular ring. This is an example of how a high resolution view
completely changes our image of the H_2_ distribution. As seen in Fig. 1,
the CO(1-0) and CO(2-1) antenna temperatures peak at 30" from the
nucleus. This galaxy is discussed in detail by Braine et al. (in prep.).

11. 1985AnTok..202.335T
Re:KUG 1223+315
S galaxy with well-developed knotty arms. In [1983AnTok..192.440T]
this galaxy is designated as KUG 1223+314.

12. 1976RC2...C...0000d
Re:NGC 4414
SN 1974G
IAU Circ. No.2664, 1974.
IAU Circ. No.2666, 1974.
IAU Circ. No.2668, 1974.
IAU Circ. No.2671, 1974.
IAU Circ. No.2674, 1974.
IAU Circ. No.2678, 1974.
Mitt. Ver. Sterne Sonneberg, 6, 155, 1974.

13. 1975ByuO...47....1A
Re:ARK 365
(= NGC 4414)
Galaxy is an Sc.
Radial velocity = +715 km/sec [HMS 1956].
Red color.

14. 1973UGC...C...0000N
Re:UGC 07539
SA(rs)c? (de Vaucouleurs), Sc- (Holmberg)

15. 1964RC1...C...0000d
Re:NGC 4414
Bright diffuse nucleus in a bright bulge. Many filamentary, partially
resolved arms with dark lanes and many branches.
See also HA, 105, 231, 1937.

16. 1918PLicO..13....9C
Re:NGC 4414
Moderately bright spiral 3' x 1.5' in p.a. 2.0^deg^. Some evidence of absorption
effects on the eastern side. A star of magn. 15 near the nucleus. See Abs. Eff.


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